Fig. 10
Comparison of various empirical WLR: this work (solid and dashed black lines are for early BSGs and mid- or late-type BSGs, respectively), Herrero et al. (2002, solid green line), Searle et al. (2008, solid cyan line), and Mokiem et al. (2007, magenta solid line). The theoretical WLR of Vink (2000) is in blue, solid and dashed lines are for Teff > 27 500 K and Teff < 22 500 K, respectively. The figure includes the sample of stars shown in Fig. 8.
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